J/ApJ/913/53 Gas content of the dwarf gal. within 2Mpc of the MW (Putman+, 2021)
The gas content and stripping of local group dwarf galaxies.
Putman M.E., Zheng Y., Price-Whelan A.M., Grcevich J., Johnson A.C.,
Tollerud E., Peek J.E.G.
<Astrophys. J., 913, 53 (2021)>
=2021ApJ...913...53P 2021ApJ...913...53P
ADC_Keywords: Galaxies, nearby; H I data; Intergalactic medium
Keywords: Local Group ; Dwarf galaxies ; Galaxy quenching ;
Circumgalactic medium ; Interstellar medium ;
Intergalactic medium ; Andromeda Galaxy ; Milky Way Galaxy
Abstract:
The gas content of the complete compilation of Local Group dwarf
galaxies (119 within 2Mpc) is presented using HI survey data. Within
the virial radius of the Milky Way (224kpc here), 53 of 55 dwarf
galaxies are devoid of gas to limits of MHI<104M☉. Within
the virial radius of M31 (266kpc), 27 of 30 dwarf galaxies are devoid
of gas (with limits typically <105M☉). Beyond the virial radii
of the Milky Way and M31, the majority of the dwarf galaxies have
detected HI gas and HI masses higher than the limits. When the
relationship between gas content and distance is investigated using a
Local Group virial radius, more of the nondetected dwarf galaxies are
within this radius (85±1 of the 93 nondetected dwarf galaxies) than
within the virial radii of the Milky Way and M31. Using the Gaia
proper-motion measurements available for 38 dwarf galaxies, the
minimum gas density required to completely strip them of gas is
calculated. Halo densities between 10-5 and 5x10-4cm-3 are
typically required for instantaneous stripping at perigalacticon. When
compared to halo density with radius expectations from simulations and
observations, 80% of the dwarf galaxies with proper motions are
consistent with being stripped by ram pressure at Milky Way
pericenter. The results suggest that a diffuse gaseous galactic halo
medium is important in quenching dwarf galaxies, and that a Local
Group medium also potentially plays a role.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 120 119 Dwarf galaxies within 2Mpc: positions and
HI parameters
table2.dat 74 119 Dwarf galaxies within 2Mpc: other parameters
table3.dat 116 38 Median orbital parameters and halo densities
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/131/332 : Velocities of individual stars in NGC 205 (Geha+, 2006)
J/AJ/133/715 : Dwarf galaxies of the Local Group (Whiting+, 2007)
J/ApJ/675/201 : Radial velocities of stars near Leo I (Mateo+, 2008)
J/ApJ/758/11 : Bayesian distances to M31 satellites (Conn+, 2012)
J/AJ/144/134 : LITTLE THINGS survey of nearby dwarf gal. (Hunter+, 2012)
J/AJ/144/4 : Dwarf galaxies in the Local Group (McConnachie+, 2012)
J/AJ/145/101 : Updated nearby galaxy catalog (Karachentsev+, 2013)
J/MNRAS/445/2061 : Absorption in multiphase CGM (Liang+, 2014)
J/ApJ/809/146 : SDSS-DR8 isolated low-mass galaxies (Bradford+, 2015)
J/ApJ/812/158 : Leo P RR Lyrae candidates & cumulative SFH (McQuinn+, 2015)
J/A+A/594/A116 : HI4PI spectra and column density maps (HI4PI team+, 2016)
J/MNRAS/458/L59 : Draco II stars gi magnitude & RVs (Martin+, 2016)
J/ApJ/827/89 : HST imaging of Pisces A and B (Tollerud+, 2016)
J/A+A/585/A41 : EBHIS spectra and HI column density maps (Winkel+, 2016)
J/MNRAS/466/2006 : Phoenix dwarf galaxy RV and [Fe/H] catalog (Kacharov+, 2017)
J/A+A/607/A48 : AGN data and absorption-line measurements (Richter+, 2017)
J/A+A/612/A26 : Deep HI observations of Leo T with WSRT (Adams+, 2018)
J/A+A/616/A12 : Gaia DR2 sources in GC and dSph (Gaia Collaboration+, 2018)
J/MNRAS/479/5343 : Nearby dwarf galaxy in Magellanic bridge (Koposov+, 2018)
J/MNRAS/478/1611 : Local Volume H I Survey (LVHIS) (Koribalski+, 2018)
J/ApJS/234/2 : The GALFA-HI survey data release 2 (Peek+, 2018)
J/ApJ/863/89 : Gaia DR2 PMs of stars in MW satellites (Simon, 2018)
J/ApJ/879/22 : GALFA-HI search for local dwarf galaxies (Defelippis+, 2019)
J/ApJ/887/115 : Sp. of stars in Price-Whelan 1 association (Nidever+, 2019)
J/ApJ/875/77 : PMs of MW satellites with Gaia & DES (Pace+, 2019)
J/ApJS/240/15 : HST/COS UV obs. of low-z SDSS galaxy groups (Stocke+, 2019)
J/MNRAS/491/3496 : Andromeda XIX member stars (Collins+, 2020)
J/ApJ/900/9 : AMIGA: Circumgalactic Medium of Andromeda (Lehner+, 2020)
J/ApJ/892/137 : Spectroscopy of Grus II, Tuc IV and Tuc V (Simon+, 2020)
J/A+A/635/A152 : Tucana dSph galaxy spectroscopic dataset (Taibi+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Dwarf galaxy name
19- 20 I2 --- f_Name ? Notes or flags on Name (1)
22- 23 I2 h RAh Hour of Right Ascension (J2000) (2)
25- 26 I2 min RAm Minute of Right Ascension (J2000)
28- 29 I2 s RAs Second of Right Ascension (J2000)
31- 31 A1 --- DE- Sign of the Declination (J2000) (2)
32- 33 I2 deg DEd Degree of Declination (J2000) (2)
35- 36 I2 arcmin DEm Arcminute of Declination (J2000)
38- 39 I2 arcsec DEs Arcsecond of Declination (J2000)
41- 44 I4 km/s Vel [-558/477]? Velocity
46- 49 I4 kpc Dist [22/1950] Distance
51- 55 F5.1 kpc e_Dist [0.4/205] Lower (or symmetric) uncertainty
in Dist
57- 59 I3 kpc E_Dist [5/152]? Upper uncertainty in Dist
61- 66 A6 --- Data Data (3)
68- 78 A11 --- Method Method (4)
80- 84 F5.1 mK sigHI [0.9/360]? 1σ HI flux (5)
86- 86 A1 --- l_MHI Limit flag on MHI
88- 94 A7 Msun MHI HI mass
96-103 A8 Msun e_MHI Lower (or symmetric) uncertainty in MHI
105-111 A7 Msun E_MHI Upper uncertainty in MHI
113-114 I2 --- rPos [5/21] Reference for RA/DE positions (6)
116-117 I2 --- r_Vel [5/27]? Reference for Vel (6)
119-120 I2 --- r_Dist [5/18] Reference for Dist (6)
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Note (1): Notes or flags on Galaxy as follows:
8 = The limit is only for the core of this tidally extended galaxy;
11 = The limit is calculated with twice the median flux in the region of
the galaxy due to strong Galactic contamination (see text);
14 = Sculptor has been claimed as a detection in previous publications,
but the HI clouds are offset from the stellar position of the galaxy
and there is abundant surrounding emission at similar velocities;
19 = Fornax is at velocities that confuse any associated HI with
Galactic emission. The limit at the stellar position and velocity is
given;
20 = This galaxy is unlikely to exist based on observations by
Cantu+ (2021ApJ...916...81C 2021ApJ...916...81C);
22 = Phoenix has confusion with Galactic emission, but the HI cloud is
at the position and velocity of the stellar component;
24 = Lacerta I is Andromeda XXXI in McConnachie (2012, J/AJ/144/4);
25 = Perseus I is Andromeda XXXIII in McConnachie (2012, J/AJ/144/4);
26 = Cassiopeia III is Andromeda XXXII in McConnachie (2012, J/AJ/144/4).
Note (2): In table 1, coordinates for Virgo I (12 00 10 +00 40 48) are very
likely a misprint for 12 00 10 -00 40 48 (see the discovery Paper;
Homma et al. 2016ApJ...832...21H 2016ApJ...832...21H); corrected at CDS.
Note (3): HI data source as follows:
GALFA1 = GALFA-HI DR1, Peek et al. (2011ApJS..194...20P 2011ApJS..194...20P);
GALFA2 = GALFA-HI DR2, Peek et al. (2018, J/ApJS/234/2);
HI4PI = HI4PI Collaboration et al. (2016, J/A+A/594/A116).
Note (4): Method as follows:
Res. = sigHI was obtained with a method consistent with the source
being resolved
Unres. = sigHI was obtained with a method consistent with the source
being unresolved
Unres. No V = the source does not have a velocity. Then the
sigHI is an average from all of the channels without
significant Galactic emission.
For HI4PI resolved, the sigHI values tend to be lower as they are the
standard deviation of the flux sum divided by the area of the optical
galaxy for 9 regions surrounding the galaxy (see text).
Note (5): The HI mass is calculated using 5σ, the noted distance, and
a fixed velocity width of 10km/s. The errors are from the distance
errors shown.
Note (6): Positions, Vel and Dist references as follows:
5 = McConnachie (2012, J/AJ/144/4).
6 = Simon (2019ARA&A..57..375S 2019ARA&A..57..375S);
7 = Luque et al. (2017MNRAS.468...97L 2017MNRAS.468...97L) for the position;
9 = Koposov et al. (2018, J/MNRAS/479/5343) for the position;
10 = Torrealba et al. (2018MNRAS.475.5085T 2018MNRAS.475.5085T) for the position;
12 = Drlica-Wagner et al. (2016ApJ...833L...5D 2016ApJ...833L...5D) for the position;
13 = Simon et al. (2020, J/ApJ/892/137) for the position and velocity;
15 = Homma et al. (2016ApJ...832...21H 2016ApJ...832...21H) for the position;
16 = Torrealba et al. (2016MNRAS.463..712T 2016MNRAS.463..712T) for the position;
17 = Torrealba et al. (2016MNRAS.459.2370T 2016MNRAS.459.2370T) for the position;
18 = Torrealba et al. (2019MNRAS.488.2743T 2019MNRAS.488.2743T) for position, velocity and
distance;
21 = Homma et al. (2018PASJ...70S..18H 2018PASJ...70S..18H) for the position;
23 = Martin et al. (2014ApJ...793L..14M 2014ApJ...793L..14M);
27 = Bouchard et al. (2005AJ....130.2058B 2005AJ....130.2058B) found a velocity of 159km/s,
but we do not note that here as this could not be confirmed by
Westmeier+ (2017MNRAS.472.4832W 2017MNRAS.472.4832W) or
Koribalski+ (2018, J/MNRAS/478/1611). Koribalski+ (2018) find
emission with a similar flux and velocity width at 36km/s, so we
leave the HI mass.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Dwarf galaxy name
19- 25 E7.1 Lsun Lv [86/1500000000]? Luminosity, solar units
27- 30 I4 pc rh [14/3065]? Half-light radius, parsecs
32- 32 A1 --- l_sigma Limit flag on sigma
34- 37 F4.1 km/s sigma [1.2/92]? Stellar velocity dispersion,
σ*
39- 42 F4.1 km/s sigma2 [7.2/61]? Gas velocity dispersion (7)
44- 47 I4 kpc DMW [19/1945] Distance from the center of Milky Way
49- 52 I4 kpc DM31 [27/2209] Distance from the center of M31
54- 57 I4 kpc DLG [-271/1702] Distance from the Local Group
surface (8)
59- 61 I3 kpc DLGh [-9/56] DLG adjustment, MW mass higher (8)
63- 65 I3 kpc DLGl [-58/-3] DLG adjustment, MW mass lower (8)
67- 68 A2 --- r_Lv Reference for Lv (9)
70- 71 A2 --- r_rh Reference for rh (9)
73- 74 A2 --- r_sigma Reference for sigma (9)
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Note (7): When sigma2 (σgas) is noted it is derived directly from
the FWHM of the HI line.
Note (8): This is the distance from the Local Group surface defined in
Section 3.1, while DMW and DM31 are from the center of the MW and M31.
The DLGh value is the variation on the distance from this surface when
the Milky Way mass is higher and the M31 mass is lower. The DLGl value
is when the Milky Way mass is lower and the M31 mass is higher. The
total Local Group mass remains the same in all cases.
Note (9): Lv, rh and sigma references as follows:
5 = McConnachie (2012, J/AJ/144/4);
6 = Simon (2019ARA&A..57..375S 2019ARA&A..57..375S);
7 = σ is from Martin et al. (2016, J/MNRAS/458/L59);
8 = Properties are from Drlica-Wagner et al. (2016ApJ...833L...5D 2016ApJ...833L...5D);
9 = σ is from Carlin & Sand (2018ApJ...865....7C 2018ApJ...865....7C). No rh is given
since this galaxy is highly disrupted;
10 = σ is from Simon et al. (2020, J/ApJ/892/137);
11 = rh is from Bothun & Thompson (1988AJ.....96..877B 1988AJ.....96..877B);
12 = The LMC has a very large stellar rotation component compared to the
stellar dispersion component. Using the stellar dispersion value
(20.2km/s), would lead to a severe underestimate of the total
mass, so we use the gas dispersion calculated from the FWHM of the
HI line;
13 = Properties are from Homma et al. (2016ApJ...832...21H 2016ApJ...832...21H);
14 = Properties are from Torrealba et al. (2019MNRAS.488.2743T 2019MNRAS.488.2743T);
15 = Properties are from Homma et al. (2018PASJ...70S..18H 2018PASJ...70S..18H);
16 = σ* is from Kacharov et al. (2017, J/MNRAS/466/2006);
17 = σ* is from Martin et al. (2014ApJ...793L..14M 2014ApJ...793L..14M);
18 = σ* is from Namumba et al. (2019MNRAS.490.3365N 2019MNRAS.490.3365N);
19 = rh is from Martin et al. (2016ApJ...824L...5M 2016ApJ...824L...5M). σ* is from
Collins et al. (2020, J/MNRAS/491/3496);
20 = σ* is from Taibi et al. (2020, J/A+A/635/A152);
21 = σ* is from Sand et al. (2015ApJ...812L..13S 2015ApJ...812L..13S);
22 = σ* is from Barnes et al. (2001MNRAS.322..486B 2001MNRAS.322..486B);
23 = σ* is from Namumba et al. (2018MNRAS.478..487N 2018MNRAS.478..487N);
24 = σ* is from Bernstein-Cooper et al. (2014AJ....148...35B 2014AJ....148...35B).
rh in this case is the semi-major axis noted by
McQuinn+ (2015, J/ApJ/812/158);
25 = σ* is from Begum et al. (2005A&A...433L...1B 2005A&A...433L...1B);
26 = σ* is from Bouchard et al. (2005AJ....130.2058B 2005AJ....130.2058B) and is
consistent with the detection at the lower velocity by
Koribalski+ (2018, J/MNRAS/478/1611);
27 = σ* is from Koribalski et al. (2018MNRAS.478.1611K 2018MNRAS.478.1611K).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Dwarf galaxy name
19 A1 --- f_Name Notes or flags on Name (1)
21- 23 I3 kpc rperi [3/417] Dwarf galaxy perigalacticon
25- 28 F4.1 kpc E_rperi [0.3/85] Upper uncertainty in rperi
30- 34 F5.1 kpc e_rperi [0.3/115] Lower uncertainty in rperi
36- 38 I3 km/s vperi [214/955] Dwarf galaxy velocity at
perigalacticon
40- 42 I3 km/s e_vperi [9/471] Uncertainty in vperi
44- 50 E7.1 cm-3 nhalo-peri [3.5e-7/0.0009] Minimum MW halo gas density
(2)
52- 59 E8.1 cm-3 E_nhalo-peri [1e-6/0.0007] Upper uncertainty in
nhalo-peri
61- 67 E7.1 cm-3 e_nhalo-peri [3e-7/0.0004] Lower uncertainty in
nhalo-peri
69- 72 I4 kpc rapo [37/3865] Dwarf galaxy apogalacticon
74- 77 I4 kpc E_rapo [4/2033] Upper uncertainty in rapo
79- 82 I4 kpc e_rapo [3/1814] Lower uncertainty in rapo
84- 86 I3 km/s vapo [34/931] Dwarf galaxy velocity at
apogalacticon
88- 90 I3 km/s e_vapo [5/482] Uncertainty in vapo
92- 98 E7.1 cm-3 nhalo-apo [9.3e-6/0.006] Minimum MW halo gas density
(2)
100- 108 E9.1 cm-3 E_nhalo-apo [6e-5/0.02] Upper uncertainty in nhalo-apo
110- 116 E7.1 cm-3 e_nhalo-apo [8.6e-6/0.004] Lower uncertainty in
nhalo-apo
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Note (1): Notes on individual galaxies as follows:
2 = This galaxy is not included in Figures 8 and 9 because of
its very small pericenter;
3 = Phoenix is the only dwarf galaxy in this list with gas.
Note (2): This is the median MW halo gas density required to strip the dwarf
galaxy at perigalacticon/apogalacticon
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Nov-2022